pypeit.sensfunc module

Implements the objects used to construct sensitivity functions.

class pypeit.sensfunc.IRSensFunc(spec1dfile, sensfile, par, par_fluxcalib=None, debug=False, chk_version=True)

Bases: SensFunc

Determine a sensitivity functions from standard-star spectra. Should only be used with NIR spectra (\(\lambda > 7000\) angstrom).

Parameters:

• spec1dfile (str) – PypeIt spec1d file for the standard file.

• sensfile (str) – File name for the sensitivity function data.

• par (SensFuncPar, optional) – The parameters required for the sensitivity function computation.

• debug (bool, optional) – Run in debug mode.

_algorithm = 'IR'

Algorithm used for the sensitivity calculation.

compute_zeropoint()

Calls routine to compute the sensitivity function.

Returns:

TelObj – Best-fitting telluric model

Return type:

Telluric

eval_zeropoint(wave, iorddet)

Evaluate the sensitivity function zero-points

Parameters:

• wave (numpy.ndarray, shape is (nspec)) – Wavelength array

• iorddet (int) – Order or detector (0-indexed)

Returns:

zeropoint

Return type:

numpy.ndarray, shape is (nspec,)

class pypeit.sensfunc.SensFunc(spec1dfile, sensfile, par, par_fluxcalib=None, debug=False, chk_version=True)

Bases: DataContainer

Base class for generating sensitivity functions from a standard-star spectrum.

This class should not be instantated by itself; instead instantiate either UVISSensFunc or IRSensFunc, depending on the wavelength range of your data (UVIS for \(\lambda < 7000\) angstrom, IR for \(\lambda > 7000\) angstrom.)

The datamodel attributes are:

Version: 1.0.2

Attribute	Type	Array Type	Description
PYP_SPEC	str		PypeIt spectrograph name
airmass	float		Airmass of the observation
algorithm	str		Algorithm used for the sensitivity calculation.
exptime	float		Exposure time
extr	str		Extraction method used for the standard star (OPT or BOX)
pypeline	str		PypeIt pipeline reduction path
sens	astropy.table.table.Table		Table with the sensitivity function
spec1df	str		PypeIt spec1D file used to for sensitivity function
std_cal	str		File name (or shorthand) with the standard flux data
std_dec	float		DEC of the standard source
std_name	str		Type of standard source
std_ra	float		RA of the standard source
telluric	Telluric		Telluric model; see Telluric
throughput	numpy.ndarray	float	Spectrograph throughput measurements
wave	numpy.ndarray	float	Wavelength vectors
zeropoint	numpy.ndarray	float	Sensitivity function zeropoints

Parameters:

• spec1dfile (str) – PypeIt spec1d file for the standard file.

• sensfile (str) – File name for the sensitivity function data.

• par (SensFuncPar) – The parameters required for the sensitivity function computation.

• par_fluxcalib (FluxCalibratePar, optional) – The parameters required for flux calibration. These are only used for flux calibration of the standard star spectrum for the QA plot. If None, defaults will be used.

• debug (bool, optional) – Run in debug mode, sending diagnostic information to the screen.

_algorithm = None

Algorithm used for the sensitivity calculation.

_bundle()

Bundle the object for writing using to_hdu().

compute_throughput()

Compute the spectroscopic throughput

Returns:

• throughput (numpy.ndarray, float, shape is (nspec, norders)) – Throughput measurements

• throughput_splice (numpy.ndarray, float, shape is (nspec_splice, norders)) – Throughput measurements for spliced spectra

compute_zeropoint()

Dummy method overloaded by subclasses

datamodel = {'PYP_SPEC': {'descr': 'PypeIt spectrograph name', 'otype': <class 'str'>}, 'airmass': {'descr': 'Airmass of the observation', 'otype': <class 'float'>}, 'algorithm': {'descr': 'Algorithm used for the sensitivity calculation.', 'otype': <class 'str'>}, 'exptime': {'descr': 'Exposure time', 'otype': <class 'float'>}, 'extr': {'descr': 'Extraction method used for the standard star (OPT or BOX)', 'otype': <class 'str'>}, 'pypeline': {'descr': 'PypeIt pipeline reduction path', 'otype': <class 'str'>}, 'sens': {'descr': 'Table with the sensitivity function', 'otype': <class 'astropy.table.table.Table'>}, 'spec1df': {'descr': 'PypeIt spec1D file used to for sensitivity function', 'otype': <class 'str'>}, 'std_cal': {'descr': 'File name (or shorthand) with the standard flux data', 'otype': <class 'str'>}, 'std_dec': {'descr': 'DEC of the standard source', 'otype': <class 'float'>}, 'std_name': {'descr': 'Type of standard source', 'otype': <class 'str'>}, 'std_ra': {'descr': 'RA of the standard source', 'otype': <class 'float'>}, 'telluric': {'descr': 'Telluric model; see :class:`~pypeit.core.telluric.Telluric`', 'otype': <class 'pypeit.core.telluric.Telluric'>}, 'throughput': {'atype': <class 'float'>, 'descr': 'Spectrograph throughput measurements', 'otype': <class 'numpy.ndarray'>}, 'wave': {'atype': <class 'float'>, 'descr': 'Wavelength vectors', 'otype': <class 'numpy.ndarray'>}, 'zeropoint': {'atype': <class 'float'>, 'descr': 'Sensitivity function zeropoints', 'otype': <class 'numpy.ndarray'>}}

DataContainer datamodel.

static empty_sensfunc_table(norders, nspec, nspec_in, ncoeff=1)

Construct an empty astropy.table.Table for the sensitivity function.

Parameters:

• norders (int) – The number of slits/orders on the detector.

• nspec (int) – The number of spectral pixels for the zeropoint arrays.

• nspec_in (int) – The number of spectral pixels on the detector for the input standard star spectrum.

• ncoeff (int, optional) – Number of coefficients for smooth model fit to zeropoints

Returns:

Instance of the empty sensitivity function table.

Return type:

astropy.table.Table

eval_zeropoint(wave, iorddet)

Dummy method, overloaded by subclasses

extrapolate(samp_fact=1.5)

Extrapolates the sensitivity function to cover an extra wavelength range set by the extrapl_blu and extrap_red parameters. This is important for making sure that the sensitivity function can be applied to data with slightly different wavelength coverage etc.

Parameters:

samp_fact (float) – Parameter governing the sampling of the wavelength grid used for the extrapolation.

Returns:

• wave_extrap (numpy.ndarray) – Extrapolated wavelength array

• zeropoint_extrap (numpy.ndarray) – Extrapolated sensitivity function

flux_std()

Flux the standard star and add it to the sensitivity function table

classmethod from_hdu(hdu, hdu_prefix=None, chk_version=True)

Instantiate the object from an HDU extension.

This overrides the base-class method, essentially just to handle the fact that the ‘TELLURIC’ extension is not called ‘MODEL’.

Parameters:

• hdu (astropy.io.fits.HDUList, astropy.io.fits.ImageHDU, astropy.io.fits.BinTableHDU) – The HDU(s) with the data to use for instantiation.

• hdu_prefix (str, optional) – Maintained for consistency with the base class but is not used by this method.

• chk_version (bool, optional) – If True, raise an error if the datamodel version or type check failed. If False, throw a warning only.

classmethod get_instance(spec1dfile, sensfile, par, par_fluxcalib=None, debug=False, chk_version=True)

Instantiate the relevant subclass based on the algorithm provided in par.

internals = ['sensfile', 'spectrograph', 'par', 'par_fluxcalib', 'qafile', 'thrufile', 'fstdfile', 'debug', 'sobjs_std', 'wave_cnts', 'counts', 'counts_ivar', 'counts_mask', 'log10_blaze_function', 'nspec_in', 'norderdet', 'wave_splice', 'zeropoint_splice', 'throughput_splice', 'steps', 'splice_multi_det', 'meta_spec', 'std_dict', 'chk_version']

A list of strings identifying a set of internal attributes that are not part of the datamodel.

run()

Execute the sensitivity function calculations.

classmethod sensfunc_weights(sensfile, waves, ech_order_vec=None, debug=False, extrap_sens=True, chk_version=True)

Get the weights based on the sensfunc

Parameters:

• sensfile (str) – the name of your fits format sensfile

• waves (numpy.ndarray) – wavelength grid for your output weights. Shape is (nspec, norders, nexp) or (nspec, norders).

• ech_order_vec (numpy.ndarray, optional) – Vector of echelle orders. Only used for echelle data.

• debug (bool) – default=False show the weights QA

• extrap_sens (bool) – default=True Extrapolate the sensitivity function

• chk_version (bool, optional) – When reading in existing files written by PypeIt, perform strict version checking to ensure a valid file. If False, the code will try to keep going, but this may lead to faults and quiet failures. User beware!

Returns:

sensfunc weights evaluated on the input waves wavelength grid, shape = same as waves

Return type:

numpy.ndarray

splice()

Routine to splice together sensitivity functions into one global sensitivity function for spectrographs with multiple detectors extending across the wavelength direction.

Returns:

• wave_splice (numpy.ndarray, shape is (nspec_splice, 1)) – wavelength array

• zeropoint_splice (numpy.ndarray, shape is (nspec_splice, 1)) – zero-point array

version = '1.0.2'

Datamodel version.

write_QA()

Write out zeropoint QA files

class pypeit.sensfunc.UVISSensFunc(spec1dfile, sensfile, par, par_fluxcalib=None, debug=False, chk_version=True)

Bases: SensFunc

Determine a sensitivity functions from standard-star spectra. Should only be used with UVIS spectra (\(\lambda < 7000\) angstrom).

Parameters:

• spec1dfile (str) – PypeIt spec1d file for the standard file.

• sensfile (str) – File name for the sensitivity function data.

• par (SensFuncPar, optional) – The parameters required for the sensitivity function computation.

• debug (bool, optional) – Run in debug mode.

_algorithm = 'UVIS'

Algorithm used for the sensitivity calculation.

compute_zeropoint()

Calls routine to compute the sensitivity function.

eval_zeropoint(wave, iorddet)

Evaluate the sensitivity function zero-points

Parameters:

• wave (numpy.ndarray, shape is (nspec)) – Wavelength array

• iorddet (int) – Order or detector (0-indexed)

Returns:

zeropoint

Return type:

numpy.ndarray, shape is (nspec,)